CHIMPS: the13CO/C18O (J = 3 → 2) Heterodyne Inner Milky Way Plane Survey

Rigby, Andrew; Moore, T. J. T.; Plume, R.; Eden, David; Urquhart, J. S.; Thompson, M. A.; Mottram, J. C.; Brunt, Christopher M.; Butner, H. M.; Dempsey, Jessica T.; Gibson, Steven J.; Hatchell, J.; Jenness, Tim; Kuno, Nario; Longmore, S. N.; Morgan, L. K.; Polychroni, D.; Thomas, H. S.; White, G. J.; Zhu, Meiping

doi:10.1093/mnras/stv2808

Cited by 105 publications

(123 citation statements)

References 67 publications

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“…Relatively few large-scale structures have been identified to date but this is likely to increase in the future with the completion of a number of molecular line surveys (e.g. The Mopra Southern Galactic Plane Survey (Burton et al 2013) and the James Clerk Maxwell Telescopes CO Heterodyne Inner Milky Way Plane Survey (CHIMPS; Rigby et al 2016) at which point this hypothesis can be more robustly tested).…”

Section: Filamentary Structures In the Galaxymentioning

confidence: 99%

ATLASGAL: A Galaxy-wide sample of dense filamentary structures

Urquhart

Leurini

et al. 2016

A&A

115

156

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Context. Filamentary structures are ubiquitous in the interstellar medium. Investigating their connection to the large-scale structure of the Galaxy and their role in star formation is leading to a paradigm shift in our understanding of star formation. Aims. We study the properties of filamentary structures from the ATLASGAL survey, which is the largest and most sensitive systematic ground-based survey of the inner Galactic plane at submillimeter wavelengths. Methods. We use the DisPerSE algorithm to identify spatially coherent structures located across the inner-Galaxy (300• < < 60• and |b| < 1.5). As a result we produce a catalogue of ∼1800 structures; these were then independently classified by the five lead authors into one of the following types: marginally resolved, elongated structures, filaments, network of filaments and complexes. This resulted in the identification of 517 filamentary structures. We determine their physical properties and investigate their overall Galactic distribution.Results. We find that almost 70% of the total 870 µm flux associated with these structures resides in filaments and networks of filaments and we estimate that they are likely to be associated with a similar fraction of the mass. Correlating these structures with tracers of massive star formation we also find that a similar fraction of the massive star forming clumps are associated with filaments and networks of filaments, which highlights the importance of these types of structures to star formation in the Galaxy. We have determined distances, masses and physical sizes for 241 of the filamentary structures. We find a median distance of 3.8 kpc, a mean mass of a few 10 3 M , a mean length of ∼6 pc and a mass-to-length ratio of (M/L) ∼200-2000 M pc −1 . We also find that these filamentary structures are tightly correlated with the spiral arms in longitude and velocity, and that their semi-major axis is preferentially aligned parallel to the Galactic mid-plane and therefore with the direction of large-scale Galactic magnetic field. We find many examples where the dense filaments identified in ATLASGAL are associated with larger scale filamentary structures (∼100 pc), and argue that this is likely to be common, and as such these may indicate a connection between large-scale Galactic dynamics and star formation. Conclusions. We have produced a large and Galaxy-wide catalogue of dense filamentary structures that are representative of a particular size and mass range not previously well studied in the literature. Analyses of the properties and distribution of these filaments reveals that they are correlated with the spiral arms and make a significant contribution to star formation in the Galaxy. Massive star formation is ongoing within ∼20% of the filaments and is strongly correlated with the filaments with the largest mass-tolength ratios. The luminosity of the embedded sources has a similar distribution to the Galactic-wide samples of young massive stars and can therefore be considered to be representative.

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Section: Filamentary Structures In the Galaxymentioning

confidence: 99%

ATLASGAL: A Galaxy-wide sample of dense filamentary structures

Urquhart

Leurini

et al. 2016

A&A

115

156

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“…The 12 CO J=3-2 data were obtained from the CO High-Resolution Survey (COHRS) with an angular and spectral resolution of 14 ′′ and 1 km s −1 (see Dempsey et al 2013). The data of the other CO isotopes were obtained from the 13 CO/C 18 O (J=3-2) Heterodyne Inner Milky Way Plane Survey (CHIMPS), which have an angular and spectral resolution of 15 ′′ and 0.5 km s −1 (Rigby et al 2016). The intensities of both set of data are on the T * A scale, and it was used the mean detector efficiency η mb = 0.61 for the 12 CO, and η mb = 0.72 for the 13 CO and C 18 O to convert T * A to main beam brightness temperature (T mb = T * A /η mb ) (Buckle et al 2009).…”

Section: Data and Sources Selectionmentioning

confidence: 99%

Exploring the ¹³CO/C¹⁸O abundance ratio towards Galactic young stellar objects and HII regions

Areal

Paron

Peña

et al. 2018

A&A

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Aims. Determining molecular abundance ratios is important not only for the study of the Galactic chemistry but also because they are useful to estimate physical parameters in a large variety of interstellar medium environments. The CO is one of the most important molecules to trace the molecular gas in the interstellar medium, and the 13 CO/C 18 O abundance ratio is usually used to estimate molecular masses and densities of regions with moderate to high densities. Nowadays this kind of isotopes ratios are in general indirectly derived from elemental abundances ratios. We present the first 13 CO/C 18 O abundance ratio study performed from CO isotopes observations towards a large sample of Galactic sources of different nature at different locations. Methods. To study the 13 CO/C 18 O abundance ratio it was used 12 CO J=3-2 data obtained form the CO High-Resolution Survey, 13 CO and C 18 O J=3-2 data from the 13 CO/C 18 O (J=3-2) Heterodyne Inner Milky Way Plane Survey, and some complementary data extracted from the James Clerk Maxwell Telescope database. It was analyzed a sample of 198 sources composed by young stellar objects (YSOs), Hii and diffuse Hii regions as catalogued in the Red MSX Source Survey in 27 • .5 ≤ l ≤ 46 • .5 and |b| ≤ 0 • .5. Results. Most of the analyzed sources are located in the galactocentric distance range 4.0-6.5 kpc. We found that YSOs have, in average, smaller 13 CO/C 18 O abundance ratios than Hii and diffuse Hii regions. Taking into account that the gas associated with YSOs should be less affected by the radiation than in the case of the others sources, selective far-UV photodissociation of C 18 O is confirmed. The 13 CO/C 18 O abundance ratios obtained in this work are systematically lower than the predicted from the known elemental abundance relations. These results would be useful in future studies of molecular gas related to YSOs and Hii regions based on the observation of these isotopes.

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“…Another interarm 'spur' (or 'armlet' or 'bridge') was found [29], covering 7° in galactic longitude (l = 32° to 39°) and 30 km/s in radial velocity (from V lsr = +60 to +90 km/s), located in between the Scutum arm and the Sagittarius arm.…”

Section: Armlet Spur Bridge Branchmentioning

confidence: 99%

A guided map to the spiral arms in the galactic disk of the Milky Way

Vallée

2017

Astronomical Review

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An up-to-date overview of the recent history is given, aiming is to present a helpful working guide to the literature and at the same time introduce key systems and observational results, starting from the Sun and going toward the Galactic Center and parts of the Zona Galactica Incognita, and beyond. We start by presenting an observational view of the Milky Way's disk plane (cartographic, dynamical, chemical crosscut, magnetic). This included the four long spiral arms in the disk of the Milky Way galaxy, their geometry, components, velocity, their widths and internal layers as well as onion-like ordered offsets, the central galactic bars, arm tangents, arm pitch and arm shape, arm origins near the Galactic Center, and other possible players in the spiral arm, such as the magnetic field and the dark matter content. After, we present a basic analysis of some theoretical predictions from galactic arm formation: numerical simulations or analytical theories, and observations are checked against predictions from various numerical simulations and analytical (theoretical) models.

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CHIMPS: the¹³CO/C¹⁸O (J = 3 → 2) Heterodyne Inner Milky Way Plane Survey

Cited by 105 publications

References 67 publications

ATLASGAL: A Galaxy-wide sample of dense filamentary structures

ATLASGAL: A Galaxy-wide sample of dense filamentary structures

Exploring the ¹³CO/C¹⁸O abundance ratio towards Galactic young stellar objects and HII regions

A guided map to the spiral arms in the galactic disk of the Milky Way

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CHIMPS: the13CO/C18O (J = 3 → 2) Heterodyne Inner Milky Way Plane Survey

Cited by 105 publications

References 67 publications

ATLASGAL: A Galaxy-wide sample of dense filamentary structures

ATLASGAL: A Galaxy-wide sample of dense filamentary structures

Exploring the 13CO/C18O abundance ratio towards Galactic young stellar objects and HII regions

A guided map to the spiral arms in the galactic disk of the Milky Way

Contact Info

Product

Resources

About

CHIMPS: the¹³CO/C¹⁸O (J = 3 → 2) Heterodyne Inner Milky Way Plane Survey

Exploring the ¹³CO/C¹⁸O abundance ratio towards Galactic young stellar objects and HII regions